Figure 15: Distribution of internal energy (left panel) and abundances of the ejecta (O, Si, Fe from left to right, normalized to solar) when the nonspherical shock is propagating in the O-rich layers at around ~20000 km along the pole (~1.5 s after bounce). For this model, the input neutrino luminosity is set as . Note that Fe in the right panel is the sum of , , and (from [248]).